Solar eclipse of January 24, 1925

A total solar eclipse occurred on Saturday, January 24, 1925. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. Totality was visible from southwestern and southeastern Quebec in Canada, and the United States, including Toronto, Niagara Falls and the northern part of New York City.

Solar eclipse of January 24, 1925
Map
Type of eclipse
NatureTotal
Gamma0.8661
Magnitude1.0304
Maximum eclipse
Duration152 sec (2 m 32 s)
Coordinates40.5°N 49.6°W / 40.5; -49.6
Max. width of band206 km (128 mi)
Times (UTC)
Greatest eclipse14:54:03
References
Saros120 (56 of 71)
Catalog # (SE5000)9339

Observations
The "diamond ring" corona, as seen from New York City on January 24, 1925

It was seen in New York City. It was reported that those above 96th Street in Manhattan saw a total solar eclipse while those below 96th Street saw a partial eclipse.[1]

Visual and radio observations were conducted by researchers working with Scientific American. [2]

Solar eclipses 1924–1928

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.[3]

Saros 120

This eclipse is a part of Saros cycle 120, repeating every 18 years, 11 days, containing 71 events. The series started with partial solar eclipse on May 27, 933 AD, and reached an annular eclipse on August 11, 1059. It was a hybrid event for 3 dates: May 8, 1510, through May 29, 1546, and total eclipses from June 8, 1564, through March 30, 2033. The series ends at member 71 as a partial eclipse on July 7, 2195. The longest duration of totality was 2 minutes, 50 seconds on March 9, 1997. All eclipses in this series occurs at the Moon’s descending node.

Tritos series

This eclipse is a part of a tritos cycle, repeating at alternating nodes every 135 synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee), but groupings of 3 tritos cycles (≈ 33 years minus 3 months) come close (≈ 434.044 anomalistic months), so eclipses are similar in these groupings.

Metonic series

The metonic series repeats eclipses every 19 years (6939.69 days), lasting about 5 cycles. Eclipses occur in nearly the same calendar date. In addition, the octon subseries repeats 1/5 of that or every 3.8 years (1387.94 days).

See also
  • List of solar eclipses visible from the United Kingdom 1000–2090 AD

Notes
  1. SOLAR ECLIPSES IN HISTORY by Ken Poshedly
  2. "The Best Observed Eclipse in History". Scientific American. 132 (3): 155. 1925. Bibcode:1925SciAm.132..155.. doi:10.1038/scientificamerican0325-155. JSTOR 24978840.
  3. van Gent, R.H. "Solar- and Lunar-Eclipse Predictions from Antiquity to the Present". A Catalogue of Eclipse Cycles. Utrecht University. Retrieved 6 October 2018.

References

Further reading
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